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Abstract

When using a laser guide star (LGS) adaptive optics (AO) system, quasi-static aberrations are observed between the measured wavefronts from the LGS wavefront sensor (WFS) and the natural guide star (NGS) WFS. These LGS aberrations, which can be as much as 1200 nm RMS on the Keck II LGS AO system, arise due to the finite height and structure of the sodium layer. The LGS aberrations vary significantly between nights due to the difference in sodium structure. In this paper, we successfully model these LGS aberrations for the Keck II LGS AO system. We use this model to characterize the LGS aberrations as a function of pupil angle, elevation, sodium structure, uplink tip/tilt error, detector field of view, the number of detector pixels, and seeing. We also employ the model to estimate the LGS aberrations for the Palomar LGS AO system, the planned Keck I and the Thirty Meter Telescope (TMT) LGS AO systems. The LGS aberrations increase with increasing telescope diameter, but are reduced by central projection of the laser compared to side projection.

The normalized sodium profiles: (a) best-fit sum of 2 Gaussians for the night of January 26 2005, (b) best-fit single Gaussian for the night of January 26 2005, and (c) median profile from the University of Western Ontario LIDAR.

(a) The modeled total magnitude of the LGS low order aberrations (nm) for Keck II versus frame number of the LIDAR profile. The frames are sampled 72 seconds apart. (b) The difference in the LGS aberrations (nm) between consecutive frames.